Evaluating planetesimal bow shocks as sites for chondrule formation
— We investigate the possible formation of chondrules by planetesimal bow shocks. The formation of such shocks is modeled using a piecewise parabolic method (PPM) code under a variety of conditions. The results of this modeling are used as a guide to study chondrule formation in a one‐dimensional, f...
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| Veröffentlicht in: | Meteoritics & planetary science 2004-11, Vol.39 (11), p.1809-1821 |
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| container_title | Meteoritics & planetary science |
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| creator | CIESLA, Fred J. HOOD, Lon L. WEIDENSCHILLING, Stuart J. |
| description | — We investigate the possible formation of chondrules by planetesimal bow shocks. The formation of such shocks is modeled using a piecewise parabolic method (PPM) code under a variety of conditions. The results of this modeling are used as a guide to study chondrule formation in a one‐dimensional, finite shock wave. This model considers a mixture of chondrule‐sized particles and micron‐sized dust and models the kinetic vaporization of the solids. We found that only planetesimals with a radius of ˜1000 km and moving at least ˜8 km/s with respect to the nebular gas can generate shocks that would allow chondrule‐sized particles to have peak temperatures and cooling rates that are generally consistent with what has been inferred for chondrules. Planetesimals with smaller radii tend to produce lower peak temperatures and cooling rates that are too high. However, the peak temperatures of chondrules are only matched for low values of chondrule wavelength‐averaged emissivity. Very slow cooling ( |
| doi_str_mv | 10.1111/j.1945-5100.2004.tb00077.x |
| format | Article |
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The formation of such shocks is modeled using a piecewise parabolic method (PPM) code under a variety of conditions. The results of this modeling are used as a guide to study chondrule formation in a one‐dimensional, finite shock wave. This model considers a mixture of chondrule‐sized particles and micron‐sized dust and models the kinetic vaporization of the solids. We found that only planetesimals with a radius of ˜1000 km and moving at least ˜8 km/s with respect to the nebular gas can generate shocks that would allow chondrule‐sized particles to have peak temperatures and cooling rates that are generally consistent with what has been inferred for chondrules. Planetesimals with smaller radii tend to produce lower peak temperatures and cooling rates that are too high. However, the peak temperatures of chondrules are only matched for low values of chondrule wavelength‐averaged emissivity. Very slow cooling (<˜100s of K/hr) can only be achieved if the nebular opacity is low, which may result after a significant amount of material has been accreted into objects that are chondrule‐sized or larger, or if chondrules formed in regions of the nebula with small dust concentrations. 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The formation of such shocks is modeled using a piecewise parabolic method (PPM) code under a variety of conditions. The results of this modeling are used as a guide to study chondrule formation in a one‐dimensional, finite shock wave. This model considers a mixture of chondrule‐sized particles and micron‐sized dust and models the kinetic vaporization of the solids. We found that only planetesimals with a radius of ˜1000 km and moving at least ˜8 km/s with respect to the nebular gas can generate shocks that would allow chondrule‐sized particles to have peak temperatures and cooling rates that are generally consistent with what has been inferred for chondrules. Planetesimals with smaller radii tend to produce lower peak temperatures and cooling rates that are too high. However, the peak temperatures of chondrules are only matched for low values of chondrule wavelength‐averaged emissivity. Very slow cooling (<˜100s of K/hr) can only be achieved if the nebular opacity is low, which may result after a significant amount of material has been accreted into objects that are chondrule‐sized or larger, or if chondrules formed in regions of the nebula with small dust concentrations. Large shock waves of approximately the same scale as those formed by gravitational instabilities or tidal interactions between the nebula and a young Jupiter do not require this to match the inferred thermal histories of chondrules.</description><subject>Chondrule</subject><subject>Cooling</subject><subject>Cooling rate</subject><subject>Dust</subject><subject>Jupiter</subject><subject>Mathematical analysis</subject><subject>Metallurgy</subject><subject>Opacity</subject><subject>Planet formation</subject><subject>Shock waves</subject><subject>Temperature</subject><issn>1086-9379</issn><issn>1945-5100</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2004</creationdate><recordtype>article</recordtype><recordid>eNqVkE9P3DAQxaOqSKXAd4jKpZeEsR3HMQcktAKKWGjFH9HbyHFsyJKNFzspy7fH0SIOveGLPZ73nmZ-SfKDQE7iOVjkRBY84wQgpwBFPtQAIES-_pJsf7S-xjdUZSaZkN-S7yEsABgnrNhOZif_VDeqoe0f0lWnejOY0C5Vl9buJQ2PTj-FVIU0tPE_tc6n-tH1jR87M1XLaHT9brJlVRfM3vu9k9ydntzOfmXz32fns-N5pjivRGaN1gaMqazhTQmUWUZkwxmxoqaC8UZBZUvZFLLUtQVZKUpAV7W2haKFbthO8nOTu_LueTRhwGUbtOmmsd0YkJSC8AIEkVG6_5904Ubfx-mQUCZKSqkkUXW4UWnvQvDG4srH5f0rEsCJLy5wgogTRJz44jtfXEfz0cb80nbm9RNOvDz-cyNEDMg2AW0YzPojQPknLAUTHO-vznBeXlzMr_kp_mVvsOCR8Q</recordid><startdate>200411</startdate><enddate>200411</enddate><creator>CIESLA, Fred J.</creator><creator>HOOD, Lon L.</creator><creator>WEIDENSCHILLING, Stuart J.</creator><general>Blackwell Publishing Ltd</general><general>Wiley Subscription Services, Inc</general><scope>BSCLL</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope></search><sort><creationdate>200411</creationdate><title>Evaluating planetesimal bow shocks as sites for chondrule formation</title><author>CIESLA, Fred J. ; HOOD, Lon L. ; WEIDENSCHILLING, Stuart J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a5587-fecce0ee8fe5d6023f319d531f7b2735da08f69d496cbf098a210c8bcf4a24cd3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2004</creationdate><topic>Chondrule</topic><topic>Cooling</topic><topic>Cooling rate</topic><topic>Dust</topic><topic>Jupiter</topic><topic>Mathematical analysis</topic><topic>Metallurgy</topic><topic>Opacity</topic><topic>Planet formation</topic><topic>Shock waves</topic><topic>Temperature</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>CIESLA, Fred J.</creatorcontrib><creatorcontrib>HOOD, Lon L.</creatorcontrib><creatorcontrib>WEIDENSCHILLING, Stuart J.</creatorcontrib><collection>Istex</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Meteoritics & planetary science</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>CIESLA, Fred J.</au><au>HOOD, Lon L.</au><au>WEIDENSCHILLING, Stuart J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Evaluating planetesimal bow shocks as sites for chondrule formation</atitle><jtitle>Meteoritics & planetary science</jtitle><date>2004-11</date><risdate>2004</risdate><volume>39</volume><issue>11</issue><spage>1809</spage><epage>1821</epage><pages>1809-1821</pages><issn>1086-9379</issn><eissn>1945-5100</eissn><coden>MPSCFY</coden><abstract>— We investigate the possible formation of chondrules by planetesimal bow shocks. The formation of such shocks is modeled using a piecewise parabolic method (PPM) code under a variety of conditions. The results of this modeling are used as a guide to study chondrule formation in a one‐dimensional, finite shock wave. This model considers a mixture of chondrule‐sized particles and micron‐sized dust and models the kinetic vaporization of the solids. We found that only planetesimals with a radius of ˜1000 km and moving at least ˜8 km/s with respect to the nebular gas can generate shocks that would allow chondrule‐sized particles to have peak temperatures and cooling rates that are generally consistent with what has been inferred for chondrules. Planetesimals with smaller radii tend to produce lower peak temperatures and cooling rates that are too high. However, the peak temperatures of chondrules are only matched for low values of chondrule wavelength‐averaged emissivity. Very slow cooling (<˜100s of K/hr) can only be achieved if the nebular opacity is low, which may result after a significant amount of material has been accreted into objects that are chondrule‐sized or larger, or if chondrules formed in regions of the nebula with small dust concentrations. Large shock waves of approximately the same scale as those formed by gravitational instabilities or tidal interactions between the nebula and a young Jupiter do not require this to match the inferred thermal histories of chondrules.</abstract><cop>Oxford, UK</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1111/j.1945-5100.2004.tb00077.x</doi><tpages>13</tpages><oa>free_for_read</oa></addata></record> |
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| subjects | Chondrule Cooling Cooling rate Dust Jupiter Mathematical analysis Metallurgy Opacity Planet formation Shock waves Temperature |
| title | Evaluating planetesimal bow shocks as sites for chondrule formation |
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